High-Fidelity Fluid Modeling of Magnetic Reconnection in Astrophysical Plasmas

Magnetic reconnection is the process by which magnetic fields pointing in opposite directions interact, annihilate and transmit their energy. Modeling the dynamics of magnetic reconnection in plasmas is key to such fields as (a) predicting solar storms, (b) understanding cosmic rays, and (c) stabilizing nuclear fusion reactions. Realistic setups are too complex to formulate analytical theory, while laboratory experiments can be expensive and difficult to probe non-intrusively. Thus, robust numerical simulations are required to provide the understanding necessary for discoveries. In this collaboration between Plasma Dynamics Modeling Lab (PDML) at Stanford and Laboratoire de Physique des Plasmas (LPP) at École Polytechnique in France, we will apply a high-fidelity fluid model developed at Stanford to study magnetic reconnection in astrophysical plasmas. In particular, we are interested in studying the effect of anisotropic (direction-dependent) pressure on the transport of magnetic fields. The simulation results will be compared to a multiscale hybrid (particle-fluid) code developed at LPP. The expertise of our collaborators at LPP will also allow us to set up more physically accurate simulations and compare to experimental data. This collaboration will advance our ability to predictively model magnetic fields in plasmas.